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Hello! Galaxy Morphology, Galaxies SuperMassive Near andBlack Far Holes and all that Ajit Kembhavi IUCAA, Pune Sudhanshu Barway Yogesh Wadadekar Vinu Vikram Abhishek Rawat C.D. Ravi Kumar Habib Khushroshahi Hubble’s Tuning Fork Lenticular Bulges of lenticulars are very similar to ellipticals. Their disk are similar to those of early type spirals, but they have no spiral arms. B/T ratios, colors and spectral properties, neutral and molecular gas fraction, star formation rate, average luminosity, M/L ratio are intermediate to ellipticals and spirals. Lenticular galaxies are a morphological transition class between ellipticals and early type spirals. Surface Brightness Distribution NGC 661 V Surface Brightness Profile Bulge –Disk Decomposition UGC 1250 2 = (oi-mi)2/i2 Bulge-Disk Decomposition Morphological Parameter Correlations The Fundamental Plane log re = A log + B log Ie + c Fundamental Plane for Morphological Mix of Galaxies The Photometric Plane 2-D Correlations Ellipticals and Early Type Bulges Photometric Plane Ellipticals Early type bulges Ellipticals and Early Type Bulges Khoshroshahi etal ApJL 2000 Residuals Photometric Plane Ellipticals Lenticulars Dwarf Ellipticals Bulges Ravikumar etal AA 2006 Bulge-Disk Correlations in Lenticular Galaxies Barway etal ApJL 2007 Barway etal MN 2009 Barway etal MN 2010 Barway etal 2011 •N-body simulations indicate that the bulge component of massive (luminous) lenticulars formed from major mergers. •But bulges in the less luminous elliptical probably formed from minor mergers or accretion events. Stripping of gas from the halo and disk lead to a change in morphology. •Correlation between photometric parameters can be a signature of the formation mechanism. Luminosity Bright field lenticulars observed in the K band: 35 Barway etal 2006 Less luminous field and cluster lenticulars with 2MASS data: 49 Bedregal etal 2006 Distribution Barway BAM06 field cluster Bulge-Disk Correlation <B/T>=0.63 R=-0.57 99.9% <B/T>=0.55 R=0.6 99.9% <B/T>=0.19 Luminosity as in low-luminosity Positive correlation Differentiator lenticulars implies that they formed by the stripping of gas from spirals, whose bulges formed through secular evolution. Bulges of more luminous lenticulars have likely formed through major mergers and rapid collapse. Kormendy Relation Faint lenticulars Bright lenticulars Ellipticals x Bright lenticulars with bars - Faint lenticulars with bars Bulges of bright lenticulars and ellipticals show similar tight correlation. These bulges are therefore more virialized than those of faint lenticulars. Correlations With Sersic Index Photometric Plane bright = 0.019 faint = 0.038 Bright lenticulars: Log n = 0.15 log re – 0.06b(0) + 1.05 Sersic index and B/T ratio Bright lenticulars with low n, low b(0), low re, low B/T. These are outliers in re-rd plot. but well correlated here. Bar Fraction and Luminosity M(K)=-24.5 UGC + SDSS + 2MASS + Hyperleda, 385 galaxies Barred M(r)=-24.5 Unbarred 83% barred lenticulars belong to the faint group. Bars are found in 21% of the faint group, but in only 6% of the bright group. Faint barred galaxies occur more frequently in groups and clusters than their bright counterparts. Environmental Dependence Kormendy Relation Faint field lenticulars Faint cluster lenticulars Cluster lenticulars appear to have faded relative to field lenticulars. They could be early type spirals which have lost gas due to ram pressure stripping or galaxy harassment. Field lenticulars show clear anti-correlation. Cluster lenticulars are restricted to a limited region and show downward scatter. This is consistent with removal of gas from the disk (and bulge) in cluster lenticulars. Color-color relations for S0 galaxies UV-optical-nir colors Ellipticals – Δ Bright S0s – Faint S0s – Color-color relations for S0 galaxies UV-optical-nir colors Ellipticals – Δ Bright S0s – Faint S0s – A Mass Fundamental Plane for SuperMassive Black Holes Ferrarese & Ford 2004 SMBH Systematics All nearby galaxies with a significant bulge contain super-massive black holes The black hole mass is proportional to the bulge mass, and to the fourth power of the central velocity dispersion The relation has been extended to lower masses, as in Seyferts Ferrarese & Merritt 2000; Gebhardt etal 2000 Kormendy & Richstone 1995 Scatter 0.79 Ellipticals 0.40 Scatter 0.34 All Galaxies SMBH Host Galaxies The Fundamental Plane for SMBH Galaxies Scatter 0.068 The Mass Fundamental Plane for SMBH Scatter 0.061 Black Hole Mass from the Mass Fundamental Plane Scatter 0.19 Black Hole Mass from Fundamental Plane of Galaxies M~ Black Hole Masses for Coma Ellipticals SMBH to IMBH SMBH Ho, Green 04 Barth etal 05 Younger etal arXiv:0804.2672.v2 Self-regulated growth of SMBH via major mrgers, minor mergers and disk instabilites through simulations. Thank You re – rd Correlation Rotation and Random Motions Kormendy & Kennicutt ARAA 2004 Disk Central Surface Brightness and Scale Length Faint lenticulars Bright lenticulars Bulges of early type spirals 2-Dimensional Relations Bulge-Disk Correlation Bulge-Disk Correlation Morphological Parameters and Entropy 2-D Correlations Deviations From Photometric Plane Towards the Hyper-Plane Photometric Plane of SMBH Galaxies Kormendy Relation for SMBH Galaxies Kormendy Relation – Luminosity Classes Distribution of Sersic Index n Ellipticals and Early Type Bulges Khosroshahi et al ApJL 2000 ApJ 2001 Morphological Mix Abell clusters ellipticals 34 Coma ellipticals 42 UGC field lenticulars 37 Bulges of early type spirals 26 Bulges of late type spirals 40 Early type dwarf galaxies 128 Morphological Mix of Galaxies Ravikumar et al 2006 The Photometric Plane and Dispersion Velocity The Hyper -Plane Ellipticals Photometric Plane Photometric Plane View from the top K1 = 0.15*log n + 0.99*log re K2 = -0.06*log n + 0.01*log re -b(0) Lenticular Galaxies: Morphological GalaxiesCorrelations and Formation Mechanisms Near and Far Ajit Kembhavi IUCAA, Pune Sudhanshu Barway Yogesh Wadadekar C.D. Ravi Kumar Black Hole Search • Stellar Dynamics: Stellar motion indicative of a central massive dark object. M87, M37, Galactic Centre _________________________________________________________________ • Gas Dynamics: Rotating gas disk. on various scales M87, NGC4258 ________________________________________________ • Relativistic effects close to the dark mass. MCG 6-30-15 _________________________________________________ • Reverberation mapping and related techniques Seyfert galaxies Massive Dark Object or Black Hole? Faber-Jackson Relation Kormendy & Kennicutt ARAA 2004